Weibel Instability in Relativistic Electron-Positron Plasmas
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**Session 64 -- Pulsars**
*Display presentation, Thursday, 9:20-4:00, Heller Lounge Room*

## [64.10] Weibel Instability in Relativistic Electron-Positron Plasmas

*T.-Y.B. Yang, Y. Gallant, J. Arons (UC Berkeley), A.B. Langdon (LLNL)*
Recent one-dimensional analytical and numerical studies$^{1}$ have demonstrated efficient acceleration
of nonthermal positrons by relativistic magnetosonic shock waves in
electron-positron-proton plasmas, which are of great relevance to pulsar
wind driven nebulae. In the one-dimensional simulations$^{2}$,
electron-positron shocks yield a down stream plasma with all the momenta in
the plane perpendicular to the background magnetic field $B_0$. Plasmas with
such anisotropy
are subject to Weibel-like instabilities, and the distribution functions
tend to be isotropized by these instabilities. Depending on the time scale
of isotropization, the shock acceleration of positrons may be modified significantly when two-dimensional effects are taken into account. With this in
mind, we study the Weibel instabilities in relativistic electron-positron
plasmas. Detailed stability properties are examined over a wide range of system
parameters by linear stability analyses. Nonlinear numerical
simulations are carried out to investigate long-term evolution of
the instability. Possible applications to the relativistic shock terminating
the pulsar wind in the Crab Nebula will be briefly outlined.
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\hrule
\begin{description}
\item[$^{1}$] Hoshino, M., and Arons, J., 1991, *Physics of Fluids*, **B3**,
818.
\item[$^{2}$] Gallant, Y., Hoshino, M., Langdon, A.B., Arons, J., and Max, C.E.,
1992, *Astrophy. J.*, **391**, 73.
\end{description}

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